It is of significant importance to calculate nuclear matter
in a variety of phases with different temperature,
utilized in simulation studies of supernovae and neutron stars.
The nuclear energy density functional method at finite temperature
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is a desirable choice for studying
the inhomogeneous neutron-star matter in outer and inner crusts.
Especially, near the boundary between the inner crust and the core,
various exotic phases, “nuclear pasta”, are expected to appear.
